{
  "id": "1405.1121",
  "version": "v2",
  "published": "2014-05-06T01:32:48.000Z",
  "updated": "2014-06-19T19:19:08.000Z",
  "title": "Neutron star-black hole mergers with a nuclear equation of state and neutrino cooling: Dependence in the binary parameters",
  "authors": [
    "Francois Foucart",
    "M. Brett Deaton",
    "Matthew D. Duez",
    "Evan O'Connor",
    "Christian D. Ott",
    "Roland Haas",
    "Lawrence E. Kidder",
    "Harald P. Pfeiffer",
    "Mark A. Scheel",
    "Bela Szilagyi"
  ],
  "comment": "20 pages, 19 figures",
  "journal": "Phys. Rev. D 90, 024026 (2014)",
  "doi": "10.1103/PhysRevD.90.024026",
  "categories": [
    "astro-ph.HE",
    "gr-qc"
  ],
  "abstract": "We present a first exploration of the results of neutron star-black hole mergers using black hole masses in the most likely range of $7M_\\odot-10M_\\odot$, a neutrino leakage scheme, and a modeling of the neutron star material through a finite-temperature nuclear-theory based equation of state. In the range of black hole spins in which the neutron star is tidally disrupted ($\\chi_{\\rm BH}\\gtrsim 0.7$), we show that the merger consistently produces large amounts of cool ($T\\lesssim 1\\,{\\rm MeV}$), unbound, neutron-rich material ($M_{\\rm ej}\\sim 0.05M_\\odot-0.20M_\\odot$). A comparable amount of bound matter is initially divided between a hot disk ($T_{\\rm max}\\sim 15\\,{\\rm MeV}$) with typical neutrino luminosity $L_\\nu\\sim 10^{53}\\,{\\rm erg/s}$, and a cooler tidal tail. After a short period of rapid protonization of the disk lasting $\\sim 10\\,{\\rm ms}$, the accretion disk cools down under the combined effects of the fall-back of cool material from the tail, continued accretion of the hottest material onto the black hole, and neutrino emission. As the temperature decreases, the disk progressively becomes more neutron-rich, with dimmer neutrino emission. This cooling process should stop once the viscous heating in the disk (not included in our simulations) balances the cooling. These mergers of neutron star-black hole binaries with black hole masses $M_{\\rm BH}\\sim 7M_\\odot-10M_\\odot$ and black hole spins high enough for the neutron star to disrupt provide promising candidates for the production of short gamma-ray bursts, of bright infrared post-merger signals due to the radioactive decay of unbound material, and of large amounts of r-process nuclei.",
  "revisions": [
    {
      "version": "v2",
      "updated": "2014-06-19T19:19:08.000Z"
    }
  ],
  "analyses": {
    "subjects": [
      "04.25.dg",
      "04.40.Dg",
      "26.30.Hj",
      "98.70.-f"
    ],
    "keywords": [
      "neutron star-black hole mergers",
      "binary parameters",
      "nuclear equation",
      "consistently produces large amounts",
      "neutrino cooling"
    ],
    "tags": [
      "journal article"
    ],
    "publication": {
      "publisher": "APS",
      "journal": "Physical Review D",
      "year": 2014,
      "month": "Jul",
      "volume": 90,
      "number": 2,
      "pages": "024026"
    },
    "note": {
      "typesetting": "TeX",
      "pages": 20,
      "language": "en",
      "license": "arXiv",
      "status": "editable",
      "inspire": 1294631,
      "adsabs": "2014PhRvD..90b4026F"
    }
  }
}